We reach values \(P_{\cal R} \approx O(10^{-1}-10^{-4})\)  that will lead to PBH formation due to the collapse of the over-dense perturbations, with a mass given as a fraction \(\gamma \simeq 0.2\)  of the horizon mass at re-entry [1]}, [2]}:
\(M_{PBH} (k) &=& \gamma \frac{4 \pi }{3} \frac{\rho }{H_M^3} = \gamma \frac{4 \pi m_P^2}{H_M} \nonumber \,,\) 
